Proton and Helium Spectra from the CREAM-III Flight

Yoon, Y. S.; Anderson, Tyler; Barrau, A.; Conklin, N. B.; Coutu, S.; Derome, L.; Han, Ji Hye; Jeon, Jin-A; Kim, K. C.; Kim, M.H.; Lee, H. Y.; Lee, J.; Lee, M. H.; Lee, S. E.; Link, J. T.; Menchaca‐Rocha, A.; Mitchell, J. W.; Mognet, S. I.; Nutter, S.; Park, I. H.; Picot-Clémente, N.; Putze, A.; Seo, E. S.; Smith, Jacob; Wu, J.

doi:10.3847/1538-4357/aa68e4

Cited by 228 publications

(234 citation statements)

References 38 publications

(35 reference statements)

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“…The statistical errors are ploted as error bars while the systematic errors are showed with a band. Note that for the CREAM-III data we also add ∼ 10% uncertainties, primarily due to the uncertainty from the energy scale [18]. Our results show good agreement with the AMS-02 and PAMELA data for E k 200 GeV.…”

Section: Pos(icrc2017)1076supporting

confidence: 78%

“…The systematic error due to the unfolding procedure is estimated by varying the parametrization of the response matrix, which is found to be less than 1.5% below 100 GeV and ∼ 4.2% at 10 TeV. Figure 6 shows the preliminary proton flux as a function of kinetic energy measured with DAMPE, compared with previous measurements by PAMELA [4], ATIC-2 [3], AMS-02 [5] and CREAM-III [18]. The statistical errors are ploted as error bars while the systematic errors are showed with a band.…”

Section: Pos(icrc2017)1076mentioning

confidence: 99%

“…The spectral hardening at E k 200 GeV can be observed from our measurements, confirming the previous results. The preliminary E 2.7 k weighted flux of CR protons measured by DAMPE, compared with previous results by PAMELA [4], AMS-02 [5], ATIC-2 [3], and CREAM-III [18]. The error bars represent statistical errors and the grey band shows the systematic errors.…”

Section: Pos(icrc2017)1076mentioning

confidence: 99%

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Studies of Cosmic-Ray Proton Flux with the DAMPE Experiment

Yue¹,

Zang²,

Dong³

et al. 2017

Proceedings of 35th International Cosmic Ray Conference — PoS(ICRC2017)

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The DArk Matter Particle Explorer (DAMPE) is a space-based mission designed as a high energy particle detector for measuring cosmic-rays and gamma-rays in space. It was successfully launched on December 17, 2015, and since then it has been in stable data taking for more than one year. The large geometric factor and thick calorimeter enables DAMPE to have very good potential to measure cosmic-rays from 20 GeV up to 100 TeV. Here we analyze the proton component using the DAMPE flight data. Comprehensive Monte-Carlo simulations have been employed to validate the event selections and estimate the efficiency as well as the geometry factor. The analysis progress is reported and discussed.

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Section: Pos(icrc2017)1076supporting

confidence: 78%

Section: Pos(icrc2017)1076mentioning

confidence: 99%

Section: Pos(icrc2017)1076mentioning

confidence: 99%

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Studies of Cosmic-Ray Proton Flux with the DAMPE Experiment

Yue¹,

Zang²,

Dong³

et al. 2017

Proceedings of 35th International Cosmic Ray Conference — PoS(ICRC2017)

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“…It should be noted that the CREAM Collaborations in [6] does not claim the detection of a softening feature, and fits the data taken in the energy interval [1,200] TeV with a simple unbroken power law obtaining a the spectral index α 2.61 ± 0.01. The CREAM paper discusses the possibility of a deviation from the power law form stating: "The spectra become softer above ∼ 20 TeV.…”

Section: Measurements Of the Cr Proton Spectrummentioning

confidence: 93%

The shape of the cosmic ray proton spectrum

Lipari

Vernetto

2020

Astroparticle Physics

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Recent observations of cosmic ray protons in the energy range 10 2 -10 5 GeV have revealed that the spectrum cannot be described by a simple power law. A hardening of the spectrum around an energy of order few hundred GeV, first observed by the magnetic spectrometers PAMELA and AMS02, has now been confirmed by several calorimeter detectors (ATIC, CREAM, CALET, NUCLEON and DAMPE). These new measurements reach higher energy and indicate that the hardening corresponds to a larger step in spectral index than what estimated by the magnetic spectrometers. Data at still higher energy (by CREAM, NUCLEON and DAMPE) show that the proton spectrum undergoes a marked softening at E ≈ 10 4 GeV. Understanding the origin of these unexpected spectral features is a significant challenge for models of the Galactic cosmic rays. An important open question is whether additional features are present in the proton spectrum between the softening and the "Knee". Extensive Air Shower detectors, using unfolding procedures that require the modeling of cosmic ray showers in the atmosphere, estimated the proton flux below and around the Knee (at E 3 PeV). These results however have large systematic uncertainties and are in poor agreement with each other. The measurement in the PeV energy range, recently presented by IceTop/IceCube, indicates a proton flux higher than extrapolations of the direct measurements calculated assuming a constant slope, and therefore requires the existence of an additional spectral hardening below the Knee. A clarification of this point is very important for an understanding of the origin of the Galactic cosmic rays, and is also essential for a precise calculation of the spectra of atmospheric neutrinos in the energy range (E 10 TeV) where they constitute the foreground for the emerging astrophysical ν signal.

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“…The live time fractions of CREAM-I, and -II were ~56% and ~75%, respectively. The trigger energy threshold was lowered from 60 MeV, used in the first two flights, to 15 MeV for CREAM-III, allowing for a significant increase in events around 1 TeV [5].…”

Section: Cream-iii Instrument and Flightmentioning

confidence: 99%

Measurement of Cosmic-Ray Nuclei with the Third Flight of the CREAM Balloon-Borne Experiment

Smith¹,

Amare²,

Anderson³

et al. 2017

Proceedings of 35th International Cosmic Ray Conference — PoS(ICRC2017)

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. CREAM-III was designed to directly measure the elemental spectra of cosmic-ray nuclei from Hydrogen to Iron in the energy range from 10 12 to 10 15 eV. Energy of incident cosmic rays was measured with a calorimeter that consisted of a densified carbon target directly above a stack of 20 alternating layers of tungsten and scintillating fiber ribbons. Multiple charge measurements were independently made with the silicon charge detector (SCD), Cherenkov Camera (CherCam), and a Timing Charge Detector (TCD) in order to identify particles and minimize backscattering effects from the calorimeter. Compared to previous CREAM flights, the electronic noise of CREAM-III was reduced, significantly lowering the energy threshold. Results from on-going analysis of the energy spectra will be presented. Conference -ICRC2017 10-20 July, 2017 Bexco, Busan, Korea † Speaker 35th International Cosmic Ray PoS(ICRC2017)198Cosmic-Ray Nuclei with CREAM-III J. R. Smith 2 1. Introduction CREAM (Cosmic Ray Energetics And Mass) is a balloon experiment designed to perform direct measurements of cosmic-ray composition and energy spectra above the atmosphere. The goal of this multi-mission experiment is to collect sufficient statistics to explore the region of energies up to 10 15 eV and test the current models of cosmic-ray acceleration and propagation in the Galaxy. The third CREAM payload (CREAM-III) was launched from McMurdo on December 19, 2007 and landed on January 17 2008, for a 29 day flight. The balloon circumnavigated the Antarctic continent twice and floated at an altitude ~38 km with an atmospheric overburden of 3.9 ± 0.4 g/cm 2 . One of the primary scientific goals of the CREAM project is the measurement of secondary cosmic-ray nuclei at high energies. Secondary nuclei are those which are produced predominantly through spallation interactions of primary nuclei, those produced in the cosmicray source regions. Because these spallation interactions are thought to occur primarily during the propagation of primary nuclei in the interstellar medium, a measurement of the ratio of secondary to primary fluxes reveals information about the propagation history (e.g., the amount of material traversed) of the primary particles In this paper, results from the on-going analysis of the data from the third flight are reported. The results presented in this paper are preliminary.

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Proton and Helium Spectra from the CREAM-III Flight

Cited by 228 publications

References 38 publications

Studies of Cosmic-Ray Proton Flux with the DAMPE Experiment

Studies of Cosmic-Ray Proton Flux with the DAMPE Experiment

The shape of the cosmic ray proton spectrum

Measurement of Cosmic-Ray Nuclei with the Third Flight of the CREAM Balloon-Borne Experiment

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